The appearance of non-spherical systems. Application to LMXB nska 1 - - PowerPoint PPT Presentation

▶
the appearance of non spherical systems application to
SMART_READER_LITE
LIVE PREVIEW

The appearance of non-spherical systems. Application to LMXB nska 1 - - PowerPoint PPT Presentation

Dec 08, 2022 316 likes •606 views

The appearance of non-spherical systems. Application to LMXB nska 1 Agata R o za ldycki 1 , Jerzy Madej 2 , Tek P. Adhikari 1 , Bei You 1 Bartosz Be 1 N. Copernicus Astronomical Center PAS, 2 Warsaw University Observatory Staszic

slide-1
SLIDE 1

The appearance of non-spherical systems. Application to LMXB

Agata R´

  • ˙

za´ nska1 Bartosz Be ldycki1, Jerzy Madej2, Tek P. Adhikari1, Bei You1

  • 1N. Copernicus Astronomical Center PAS, 2Warsaw University Observatory

Staszic Palace, 31.03.2017, Warsaw, Poland

Agata R´

  • ˙

za´ nska NewCompStar 2017 1 / 15

slide-2
SLIDE 2

Jerzy Madej

1 Professor at the University of Warsaw Agata R´

  • ˙

za´ nska NewCompStar 2017 2 / 15

slide-3
SLIDE 3

Jerzy Madej

1 Professor at the University of Warsaw 2 1983 awarded by Ministry of Science for the best PhD Agata R´

  • ˙

za´ nska NewCompStar 2017 2 / 15

slide-4
SLIDE 4

Jerzy Madej

1 Professor at the University of Warsaw 2 1983 awarded by Ministry of Science for the best PhD 3 MIT, USA, postdoc 1 year Agata R´

  • ˙

za´ nska NewCompStar 2017 2 / 15

slide-5
SLIDE 5

Jerzy Madej

1 Professor at the University of Warsaw 2 1983 awarded by Ministry of Science for the best PhD 3 MIT, USA, postdoc 1 year 4 CITA, University of Toronto, postdoc 1 year Agata R´

  • ˙

za´ nska NewCompStar 2017 2 / 15

slide-6
SLIDE 6

Radiative transfer equation

Radiation through a foggy atmosphere,

  • A. Schuster, 1905, ApJ, 21, 1.

Agata R´

  • ˙

za´ nska NewCompStar 2017 3 / 15

slide-7
SLIDE 7

Radiative transfer equation

Radiation through a foggy atmosphere,

  • A. Schuster, 1905, ApJ, 21, 1.

Agata R´

  • ˙

za´ nska NewCompStar 2017 3 / 15

slide-8
SLIDE 8

Radiative transfer equation

µ dIν dτν = Iν − jν κν + σν = Iν − Sν Emission coefficient jν is the sum

  • f three terms, jν = jth

ν + jsc ν + jfl ν .

Agata R´

  • ˙

za´ nska NewCompStar 2017 4 / 15

slide-9
SLIDE 9

Radiative transfer equation

µ dIν dτν = Iν − jν κν + σν = Iν − Sν Emission coefficient jν is the sum

  • f three terms, jν = jth

ν + jsc ν + jfl ν .

Requires iteration with gas(X,Y,Z) structure due to equilibrium equations: Hydrostatic equil. => dP

dz

Agata R´

  • ˙

za´ nska NewCompStar 2017 4 / 15

slide-10
SLIDE 10

Radiative transfer equation

µ dIν dτν = Iν − jν κν + σν = Iν − Sν Emission coefficient jν is the sum

  • f three terms, jν = jth

ν + jsc ν + jfl ν .

Requires iteration with gas(X,Y,Z) structure due to equilibrium equations: Hydrostatic equil. => dP

dz

Radiative equil. => dT

dz

Agata R´

  • ˙

za´ nska NewCompStar 2017 4 / 15

slide-11
SLIDE 11

Radiative transfer equation

µ dIν dτν = Iν − jν κν + σν = Iν − Sν Emission coefficient jν is the sum

  • f three terms, jν = jth

ν + jsc ν + jfl ν .

Requires iteration with gas(X,Y,Z) structure due to equilibrium equations: Hydrostatic equil. => dP

dz

Radiative equil. => dT

dz

EoS - usually ideal gas

Agata R´

  • ˙

za´ nska NewCompStar 2017 4 / 15

slide-12
SLIDE 12

Model atmosphere calculations - glossary of terms

1 Specific intensity Iν, which flows through one cm2 on the

surface of an emitter into a direction. It is an intrinsic property of the source in erg cm−2 s−1 Hz−1 sr−1.

Agata R´

  • ˙

za´ nska NewCompStar 2017 5 / 15

slide-13
SLIDE 13

Model atmosphere calculations - glossary of terms

1 Specific intensity Iν, which flows through one cm2 on the

surface of an emitter into a direction. It is an intrinsic property of the source in erg cm−2 s−1 Hz−1 sr−1.

2 Energy dependent flux is the average of Iν weighted by cos θ

(zenithal angle). Integration is over full solid angle 4π: Fν =

  • Iνdω

It is an intrinsic property of the source in erg cm−2 s−1 Hz−1.

Agata R´

  • ˙

za´ nska NewCompStar 2017 5 / 15

slide-14
SLIDE 14

Model atmosphere calculations - glossary of terms

1 Specific intensity Iν, which flows through one cm2 on the

surface of an emitter into a direction. It is an intrinsic property of the source in erg cm−2 s−1 Hz−1 sr−1.

2 Energy dependent flux is the average of Iν weighted by cos θ

(zenithal angle). Integration is over full solid angle 4π: Fν =

  • Iνdω

It is an intrinsic property of the source in erg cm−2 s−1 Hz−1.

3 Infinitesimal energy dFν can be measured by a distant

  • bserver in flat space, over infinitesimal part of full solid angle

dFν = Iνdω, subtended by the area as seen by an observer. It is NOT an intrinsic property of the source in erg cm−2 s−1 Hz−1.

Agata R´

  • ˙

za´ nska NewCompStar 2017 5 / 15

slide-15
SLIDE 15

Spherically symmetric stars - ideal model of NS

RNS r

θ

To Observer

Fν,NS = 2π

RNS

D

2 1

Iνµdµ =

RNS

D

2

Fν The observed intensity per detector area is proportional to the flux emitted locally from 1 cm2 of the star’s surface, only due to the spherical shape of the emitting region. Mihalas 1976.

Agata R´

  • ˙

za´ nska NewCompStar 2017 6 / 15

slide-16
SLIDE 16

Axially symmetric accretion disk - Shakura & Sunyaev 1973

θ′

Rin Rout R To Observer

Fν,AD =

  • Ω

Iνdω = 2πsin θ′ D2

Rout

Rin

IνRdR, Monochromatic intensity, Iν emitted in the specific direction is integrated over the disk surface from the inner to outer disk radii.

Agata R´

  • ˙

za´ nska NewCompStar 2017 7 / 15

slide-17
SLIDE 17

LMXB - neutron star with the accretion disk

Ω

Accretion disk Accretion disk Neutron Star Rout Hdisk

Obs.

Rboost Neutron star

MNS = 1.4M⊙ RNS = 12 km

line of sight Accretion disk Accretion disk

θ′ θ′ i

Rin = 3RSchw Hdisk

1 2 4 5

Fν,All = π

RNS

D

2 1

Iνµdµ +

1

cos θ′

Iνµdµ

  • +

2 D2

RNS

Iν sin θ′ R2

NS − x2 dx −

RNS sin θ′

Iν

  • R2

NS sin2 θ′ − x2 dx

  • +

π sin θ′ D2

Rout

Rin

IνRdR +

Rout

Rboost

IνRdR

  • ,

Agata R´

  • ˙

za´ nska NewCompStar 2017 8 / 15

slide-18
SLIDE 18

LMXB at different viewing angles

10-2 10-1 100 101 θ′ =10 ◦ θ′ =30 ◦ θ′ =90 ◦ ˙ m =0.0008, Teff,NS =4.0 ×106 K ˙ m =0.05, Teff,NS =1.6 ×107 K 10-2 10-1 100 101 102 E*PhE [keV s−1 cm−2 keV−1 ] θ′ =10 ◦ θ′ =30 ◦ θ′ =90 ◦ ˙ m =0.003, Teff,NS =6.3 ×106 K ˙ m =0.2, Teff,NS =2.5 ×107 K 10-2 10-1 100 101 E [keV] 10-1 100 101 102 103 θ′ =10 ◦ θ′ =30 ◦ θ′ =90 ◦ ˙ m =0.01, Teff,NS =1.0 ×107 K ˙ m =0.8, Teff,NS =4.0 ×107 K 10-1 100 101 ˙ m =0.001, Teff,NS =1.6 ×107 K Fν,NS θ′ =10 ◦ θ′ =30 ◦ θ′ =50 ◦ θ′ =70 ◦ θ′ =90 ◦ 100 101 102 E*PhE [keV s−1 cm−2 keV−1 ] ˙ m =0.02, Teff,NS =2.5 ×107 K Fν,NS θ′ =10 ◦ θ′ =30 ◦ θ′ =50 ◦ θ′ =70 ◦ θ′ =90 ◦ 10-2 10-1 100 101 E [keV] 101 102 103 ˙ m =0.4, Teff,NS =4.0 ×107 K Fν,NS θ′ =10 ◦ θ′ =30 ◦ θ′ =50 ◦ θ′ =70 ◦ θ′ =90 ◦

Agata R´

  • ˙

za´ nska NewCompStar 2017 9 / 15

slide-19
SLIDE 19

X-ray observations of XTE J1709-267 by XMM-Newton

10-3 10-2 10-1 100 101

Ene rgy [ke V]

10-6 10-5 10-4 10-3

E*PhE [keV s−1 cm−2 keV−1 ]

XTE J1709-267 MOS unfolde d da ta

T

  • ta l Mode l

Powe rla w LMXB Absorbe d LMXB Absorbe d powe rla w Agata R´

  • ˙

za´ nska NewCompStar 2017 10 / 15

slide-20
SLIDE 20

X-ray observations of XTE J1709-267 by XMM-Newton

Parameters from the fitting of XTEJ1709-267 XMM-Newton MOS1 data. The reduced χ2 of the fit is equal 1.32 Model Parameter Value Error tbabs NH 2.67 × 1021 cm−2 ±0.22 lmxb Teff,NS 6.335 × 106 K ±0.105 × 106 lmxb ˙ m 0.0104 ˙ mEdd ±0.0019 lmxb θ′ 70.6◦ – lmxb Norm. 5.33 × 10−5 ±0.27 × 10−5 powerlaw Γ 0.36 – powerlaw Norm. 1.79 × 10−5 –

Agata R´

  • ˙

za´ nska NewCompStar 2017 11 / 15

slide-21
SLIDE 21

X-ray observations of XTE J1709-267 by XMM-Newton

Parameters from the fitting of XTEJ1709-267 XMM-Newton MOS1 data. The reduced χ2 of the fit is equal 1.32 Model Parameter Value Error tbabs NH 2.67 × 1021 cm−2 ±0.22 lmxb Teff,NS 6.335 × 106 K ±0.105 × 106 lmxb ˙ m 0.0104 ˙ mEdd ±0.0019 lmxb θ′ 70.6◦ – lmxb Norm. 5.33 × 10−5 ±0.27 × 10−5 powerlaw Γ 0.36 – powerlaw Norm. 1.79 × 10−5 – Our fit is consistent with the BB fit by Degenaar et al. (2013). We

  • btained 3.5 times hotter star, but the warm absorption column is

by 0.2 smaller.

Agata R´

  • ˙

za´ nska NewCompStar 2017 11 / 15

slide-22
SLIDE 22

Summary

1 Overall continuum shape from non-spherical LMXB shows two

  • peaks. The lower energy peak is caused by the accretion disk

emission, whereas higher energy bump is due to the neutron

  • star. Published in Acta Astronomica 2017, vol. 67

Agata R´

  • ˙

za´ nska NewCompStar 2017 12 / 15

slide-23
SLIDE 23

Summary

1 Overall continuum shape from non-spherical LMXB shows two

  • peaks. The lower energy peak is caused by the accretion disk

emission, whereas higher energy bump is due to the neutron

  • star. Published in Acta Astronomica 2017, vol. 67

2 X-ray binaries: Zhang et al. 2000, GRS 19151+105 Agata R´

  • ˙

za´ nska NewCompStar 2017 12 / 15

slide-24
SLIDE 24

Summary

1 Overall continuum shape from non-spherical LMXB shows two

  • peaks. The lower energy peak is caused by the accretion disk

emission, whereas higher energy bump is due to the neutron

  • star. Published in Acta Astronomica 2017, vol. 67

2 X-ray binaries: Kolehmainer et al. 2011, GX 339-4 Agata R´

  • ˙

za´ nska NewCompStar 2017 13 / 15

slide-25
SLIDE 25

Summary

1 Seyfert galaxies: Jin et al. 2012, J112328+052823,

PG 1415+451

Agata R´

  • ˙

za´ nska NewCompStar 2017 14 / 15

slide-26
SLIDE 26

Summary

1 ULX sources Walton et al. 2015, Holmberg II X-1 Agata R´

  • ˙

za´ nska NewCompStar 2017 15 / 15

slide-27
SLIDE 27

Summary

1 ULX sources Walton et al. 2015, Holmberg II X-1

THANK YOU

Agata R´

  • ˙

za´ nska NewCompStar 2017 15 / 15